H I observations of galaxies

Gavazzi, G.; O'Neil, K.; Boselli, A.; Driel, W.D. van

doi:10.1051/0004-6361:20053844

Cited by 72 publications

(103 citation statements)

References 42 publications

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“…In this figure, we include all galaxies which have H I mass larger than 10 4 h −1 M . The magenta arrow represents the lower limit of the overall H I mass of the Coma cluster by summing H I masses of 223 H I-detected late-type galaxies in Gavazzi et al (2006). The total mass of the Coma cluster from Kubo et al (2007) is shown for comparison.…”

Section: Imprinted Photoionization Feedback On H I Clusteringmentioning

confidence: 99%

The spatial distribution of neutral hydrogen as traced by low H i mass galaxies

Kim

Wyithe

Baugh

et al. 2016

Mon. Not. R. Astron. Soc.

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The formation and evolution of galaxies with low neutral atomic hydrogen (HI) masses, M HI <10 8 h −2 M , are affected by host dark matter halo mass and photoionisation feedback from the UV background after the end of reionization. We study how the physical processes governing the formation of galaxies with low HI mass are imprinted on the distribution of neutral hydrogen in the Universe using the hierarchical galaxy formation model, GALFORM. We calculate the effect on the correlation function of changing the HI mass detection threshold at redshifts 0 z 0.5. We parameterize the clustering as ξ(r) = (r/r 0 ) −γ and we find that including galaxies with M HI <10 8 h −2 M increases the clustering amplitude r 0 and slope γ compared to samples of higher HI masses. This is due to these galaxies with low HI masses typically being hosted by haloes with masses greater than 10 12 h −1 M , and is in contrast to optically selected surveys for which the inclusion of faint, blue galaxies lowers the clustering amplitude. We show the HI mass function for different host dark matter halo masses and galaxy types (central or satellite) to interpret the values of r 0 and γ of the clustering of HI-selected galaxies. We also predict the contribution of low HI mass galaxies to the 21cm intensity mapping signal. We calculate that a dark matter halo mass resolution better than ∼10 10 h −1 M at redshifts higher than 0.5 is required in order to predict converged 21cm brightness temperature fluctuations.

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Section: Imprinted Photoionization Feedback On H I Clusteringmentioning

confidence: 99%

The spatial distribution of neutral hydrogen as traced by low H i mass galaxies

Kim

Wyithe

Baugh

et al. 2016

Mon. Not. R. Astron. Soc.

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“…It has also become clear that the physical properties of star-forming systems that inhabit rich environments, which are characterised by a reduced atomic (e.g. Cayatte et al 1990;Solanes et al 2001;Vollmer et al 2001;Gavazzi et al 2006a) and molecular gas content (Fumagalli et al 2009;Boselli et al 2014c), dust content 2012a), and star formation (e.g. Gavazzi et al 1998Gavazzi et al , 2006bGavazzi et al , 2013Lewis et al 2002;Goto et al 2003;Boselli et al 2015), are systematically different from those of their isolated analogues.…”

Section: Introductionmentioning

confidence: 99%

Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569

Boselli

Cuillandre

Fossati

et al. 2016

A&A

Self Cite

132

169

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Using MegaCam at the CFHT, we obtained a deep narrow band Hα+ [NII] wide-field image of NGC 4569 (M90), the brightest late-type galaxy in the Virgo cluster. The image reveals the presence of long tails of diffuse ionized gas, without any associated stellar component extending from the disc of the galaxy up to 80 kpc (projected distance) and with a typical surface brightness of a few 10 −18 erg s −1 cm −2 arcsec −2 . These features provide direct evidence that NGC 4569 is undergoing a ram-presure stripping event. The image also shows a prominent 8 kpc spur of ionized gas that is associated with the nucleus that spectroscopic data identify as an outflow. With some assumptions on the 3D distribution of the gas, we use the Hα surface brightness of these extended low-surface brightness features to derive the density and the mass of the gas that has been stripped during the interaction of the galaxy with the intracluster medium. The comparison with ad hoc chemo-spectrophotometric models of galaxy evolution indicates that the mass of the Hα emitting gas in the tail is a large fraction of that of the cold phase that has been stripped from the disc, suggesting that the gas is ionized within the tail during the stripping process. The lack of star-forming regions suggests that mechanisms other than photoionization are responsible for the excitation of the gas (shocks, heat conduction, magneto hydrodynamic waves). This analysis indicates that ram pressure stripping is efficient in massive (M star 10 10.5 M ) galaxies located in intermediate-mass ( 10 14 M ) clusters under formation. It also shows that the mass of gas expelled by the nuclear outflow is only ∼1% than that removed during the ram pressure stripping event. Together these results indicate that ram pressure stripping, rather than starvation through nuclear feedback, can be the dominant mechanism that is responsible for the quenching of the star formation activity of galaxies in high density environments.Key words. galaxies: individual: NGC 4569 -galaxies: clusters: general -galaxies: clusters: individual: Virgo -galaxies: evolutiongalaxies: interactions -galaxies: ISM Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canadian-French-Hawaii Telescope (CFHT) which is operated by the

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“…Tully & Shaya 1984;Colless & Dunn 1996) whose physical properties systematically change once they reach the densest regions. It is now widely recognised that late-type galaxies located in rich clusters are generally HI-deficient Gavazzi 1987;Cayatte et al 1990;Solanes et al 2001;Gavazzi et al 2005Gavazzi et al , 2006a. There is growing evidence indicating that they also lack molecular gas (Fumagalli et al 2009;Boselli et al 2014b) and dust (Cortese et al 2012a) with respect to similar Visiting astronomer at CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia. objects in the field.…”

Section: Introductionmentioning

confidence: 99%

Quenching of the star formation activity in cluster galaxies

Boselli

Roehlly

Fossati

et al. 2016

A&A

Self Cite

119

155

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We study the star formation quenching mechanism in cluster galaxies by fitting the spectral energy distribution (SED) of the Herschel Reference Survey, a complete volume-limited K-band-selected sample of nearby galaxies including objects in different density regions, from the core of the Virgo cluster to the general field. The SEDs of the target galaxies were fitted using the CIGALE SED modelling code. The truncated activity of cluster galaxies was parametrised using a specific star formation history with two free parameters, the quenching age QA and the quenching factor QF. These two parameters are crucial for the identification of the quenching mechanism, which acts on long timescales when starvation processes are at work, but is rapid and efficient when ram pressure occurs. To be sensitive to an abrupt and recent variation of the star formation activity, we combined twenty photometric bands in the UV to far-infrared in a new way with three age-sensitive Balmer line absorption indices extracted from available medium-resolution (R ∼ 1000) integrated spectroscopy and with Hα narrow-band imaging data. The use of a truncated star formation history significantly increases the quality of the fit in HI-deficient galaxies of the sample, that is to say, in those objects whose atomic gas content has been removed during the interaction with the hostile cluster environment. The typical quenching age of the perturbed late-type galaxies is QA < ∼ 300 Myr whenever the activity of star formation is reduced by 50% < QF ≤ 80% and QA < ∼ 500 Myr for QF > 80%, while that of the quiescent early-type objects is QA 1−3 Gyr. The fraction of late-type galaxies with a star formation activity reduced by QF > 80% and with an HI-deficiency parameter HI − de f > 0.4 drops by a factor of ∼5 from the inner half virial radius of the Virgo cluster (R/R vir < 0.5), where the hot diffuse X-ray emitting gas of the cluster is located, to the outer regions (R/R vir > 4). The efficient quenching of the star formation activity observed in Virgo suggests that the dominant stripping process is ram pressure. We discuss the implication of this result in the cosmological context of galaxy evolution.

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H I observations of galaxies

Cited by 72 publications

References 42 publications

The spatial distribution of neutral hydrogen as traced by low H i mass galaxies

The spatial distribution of neutral hydrogen as traced by low H i mass galaxies

Spectacular tails of ionized gas in the Virgo cluster galaxy NGC 4569

Quenching of the star formation activity in cluster galaxies

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